For GW170104, we assume uniform priors for detector-frame component masses \(m_{1,2}^{\mathrm {det}} \in \)  [5.5, 160) M\(_\odot \) . When generating the waveform in the MCMC, the masses are transformed to the detector-frame chirp mass \(\mathcal {M}^\mathrm {det}\)  and \(q\)  with a restriction \(12.3 < \mathcal {M}^\mathrm {det}/M_\odot < 45.0\) , and \(1 < q < 8\)  where \(q = \max \lbrace  m_1^{\mathrm {det}}, m_2^{\mathrm {det}} \rbrace  / \min \lbrace  m_1^{\mathrm {det}}, m_2^{\mathrm {det}} \rbrace \) . We assume uniform prior distributions \(m_{1,2}^{\mathrm {det}} \in \)  [3, 50) M\(_\odot \)  for GW170608, \(m_{1,2}^{\mathrm {det}} \in \)  [10, 90) M\(_\odot \)  for GW170729, \(m_{1,2}^{\mathrm {det}} \in \)  [10, 80) M\(_\odot \)  for GW170814, and \(m_{1,2}^{\mathrm {det}} \in \)  [5, 80) M\(_\odot \)  for GW170809, GW170818, and GW170823. For the luminosity distance, we assume a uniform in volume distribution such that \(p(d_L | H)~\propto d_L^2\) , with \(d_L \in \)  [100, 2500) Mpc for GW170104, \(d_L \in \)  [10, 1500) Mpc for GW170608, \(d_L \in \)  [10, 5000) Mpc for GW170729, \(d_L \in \)  [10, 2500) Mpc for GW170809, \(d_L \in \)  [10, 1500) Mpc for GW170814, \(d_L \in \)  [10, 3000) Mpc for GW170818, and \(d_L \in \)  [10, 5000) Mpc for GW170823. The priors for the remaining parameters are the same for all the events. For spin magnitudes, we use uniform priors \(a_{1,2} \in \)  [0.0, 0.99).
We use a uniform solid angle prior for the spin angles, assuming a uniform distribution for the spin azimuthal angles \(\theta _{1,2}^\mathrm {a} \in [0, 2\pi )\)  and a sine-angle distribution for the spin polar angles \(\theta _{1,2}^\mathrm {p}\) .
We use uniform priors for the arrival time \(t_c \in [t_s - 0.1~s, t_s + 0.1~s)\)  where \(t_s\)  is the trigger time of the event being analyzed, reported in  [1]}, [2]}, [3]}.
For the sky location parameters, we use a uniform distribution prior for \(\alpha \in [0, 2\pi )\)  and a cosine-angle distribution prior for \(\delta \) . We use a uniform prior for the polarization angle \(\psi \in [0, 2 \pi )\)  and a sine-angle distribution for the inclination angle \(\iota \)  prior. The mass and spin priors for GW170104 are the same as those mentioned for the final analysis using the “effective precession” model in Ref. [1]}.
